adsabs/AstroCLIMB huggingface dataset:
Paper: The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2
Authors: Jihye Hwang, Jongsoo Kim, Kate Pattle, Chang Won Lee, Patrick M. Koch, Doug Johnstone, Kohji Tomisaka, Anthony Whitworth, Ray S. Furuya, Ji-hyun Kang, A-Ran Lyo, Eun Jung Chung, Doris Arzoumanian, Geumsook Park, Woojin Kwon, Shinyoung Kim, Motohide Tamura, Jungmi Kwon, Archana Soam, Ilseung Han, Thiem Hoang, Kyoung Hee Kim, Takashi Onaka, Chakali Eswaraiah, Derek Ward-Thompson, Hong-Li Liu, Xindi Tang, Wen Ping Chen, Masafumi Matsumura, Thuong Duc Hoang, Zhiwei Chen, Valentin J. M. Le Gouellec, Florian Kirchschlager, Frédérick Poidevin, Pierre Bastien, Keping Qiu, Tetsuo Hasegawa, Shih-Ping Lai, Do-Young Byun, Jungyeon Cho, Minho Choi, Youngwoo Choi, Yunhee Choi, Il-Gyo Jeong, Miju Kang, Hyosung Kim, Kee-Tae Kim, Jeong-Eun Lee, Sang-Sung Lee, Yong-Hee Lee, Hyeseung Lee, Mi-Ryang Kim, Hyunju Yoo, Hyeong-Sik Yun, Mike Chen, James Di Francesco, Jason Fiege, Laura M. Fissel, Erica Franzmann, Martin Houde, Kevin Lacaille, Brenda Matthews, Sarah Sadavoy, Gerald Moriarty-Schieven, Mehrnoosh Tahani, Tao-Chung Ching, Y. Sophia Dai, Yan Duan, Qilao Gu, Chi-Yan Law, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Tie Liu, Xing Lu, Lei Qian, Hongchi Wang, Jintai Wu, Jinjin Xie, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Yapeng Zhang, Jianjun Zhou, Lei Zhu, David Berry, Per Friberg, Sarah Graves, Junhao Liu, Steve Mairs, Harriet Parsons, Mark Rawlings, Yasuo Doi, Saeko Hayashi, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Akimasa Kataoka, Koji Kawabata, Gwanjeong Kim, Masato I. N. Kobayashi, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Tae-Soo Pyo, Hiro Saito, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Yusuke Tsukamoto, Tetsuya Zenko, Huei-Ru Vivien Chen, Hao-Yuan Duan, Lapo Fanciullo, Francisca Kemper, Chin-Fei Lee, Sheng-Jun Lin, Sheng-Yuan Liu, Nagayoshi Ohashi, Ramprasad Rao, Ya-Wen Tang, Jia-Wei Wang, Meng-Zhe Yang, Hsi-Wei Yen, Tyler L. Bourke, Antonio Chrysostomou, Victor Debattista, David Eden, Stewart Eyres, Sam Falle, Gary Fuller, Tim Gledhill, Jane Greaves, Matt Griffin, Jennifer Hatchell, Janik Karoly, Jason Kirk, Vera Könyves, Steven Longmore, Sven van Loo, Ilse de Looze, Nicolas Peretto, Felix Priestley, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Giorgio Savini, Anna Scaife, Serena Viti, Pham Ngoc Diep, Nguyen Bich Ngoc, Le Ngoc Tram, Philippe André, Simon Coudé, C. Darren Dowell, Rachel Friesen, Jean-Franćois Robitaille
Figure caption: Maps of column density (left panel) and velocity dispersion (right panel). The 18″.2 resolution column density map is produced by Kumar et al. (2022) using getsf method. The velocity dispersion map is obtained by measuring the FWHMs of the nonthermal component of the C18O spectral line, observed using HARP on the JCMT. Contours are the same as those defined in Figure 3.
Paper: The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2
Authors: Jihye Hwang, Jongsoo Kim, Kate Pattle, Chang Won Lee, Patrick M. Koch, Doug Johnstone, Kohji Tomisaka, Anthony Whitworth, Ray S. Furuya, Ji-hyun Kang, A-Ran Lyo, Eun Jung Chung, Doris Arzoumanian, Geumsook Park, Woojin Kwon, Shinyoung Kim, Motohide Tamura, Jungmi Kwon, Archana Soam, Ilseung Han, Thiem Hoang, Kyoung Hee Kim, Takashi Onaka, Chakali Eswaraiah, Derek Ward-Thompson, Hong-Li Liu, Xindi Tang, Wen Ping Chen, Masafumi Matsumura, Thuong Duc Hoang, Zhiwei Chen, Valentin J. M. Le Gouellec, Florian Kirchschlager, Frédérick Poidevin, Pierre Bastien, Keping Qiu, Tetsuo Hasegawa, Shih-Ping Lai, Do-Young Byun, Jungyeon Cho, Minho Choi, Youngwoo Choi, Yunhee Choi, Il-Gyo Jeong, Miju Kang, Hyosung Kim, Kee-Tae Kim, Jeong-Eun Lee, Sang-Sung Lee, Yong-Hee Lee, Hyeseung Lee, Mi-Ryang Kim, Hyunju Yoo, Hyeong-Sik Yun, Mike Chen, James Di Francesco, Jason Fiege, Laura M. Fissel, Erica Franzmann, Martin Houde, Kevin Lacaille, Brenda Matthews, Sarah Sadavoy, Gerald Moriarty-Schieven, Mehrnoosh Tahani, Tao-Chung Ching, Y. Sophia Dai, Yan Duan, Qilao Gu, Chi-Yan Law, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Tie Liu, Xing Lu, Lei Qian, Hongchi Wang, Jintai Wu, Jinjin Xie, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Yapeng Zhang, Jianjun Zhou, Lei Zhu, David Berry, Per Friberg, Sarah Graves, Junhao Liu, Steve Mairs, Harriet Parsons, Mark Rawlings, Yasuo Doi, Saeko Hayashi, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Akimasa Kataoka, Koji Kawabata, Gwanjeong Kim, Masato I. N. Kobayashi, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Tae-Soo Pyo, Hiro Saito, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Yusuke Tsukamoto, Tetsuya Zenko, Huei-Ru Vivien Chen, Hao-Yuan Duan, Lapo Fanciullo, Francisca Kemper, Chin-Fei Lee, Sheng-Jun Lin, Sheng-Yuan Liu, Nagayoshi Ohashi, Ramprasad Rao, Ya-Wen Tang, Jia-Wei Wang, Meng-Zhe Yang, Hsi-Wei Yen, Tyler L. Bourke, Antonio Chrysostomou, Victor Debattista, David Eden, Stewart Eyres, Sam Falle, Gary Fuller, Tim Gledhill, Jane Greaves, Matt Griffin, Jennifer Hatchell, Janik Karoly, Jason Kirk, Vera Könyves, Steven Longmore, Sven van Loo, Ilse de Looze, Nicolas Peretto, Felix Priestley, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Giorgio Savini, Anna Scaife, Serena Viti, Pham Ngoc Diep, Nguyen Bich Ngoc, Le Ngoc Tram, Philippe André, Simon Coudé, C. Darren Dowell, Rachel Friesen, Jean-Franćois Robitaille
Figure caption: Map of magnetic field orientation in Mon R2. Segments are the same in the left panel of Figure 1, but are shown with a uniform length for clarity. The background gray-scale image, the yellow star, and the circle marking the beam are as those shown in Figure 1. Colored lines show the skeletons of the filaments that were obtained using the getsf algorithm (Men’shchikov 2021) by Kumar et al. (2022). The numbers of each filament are marked on each rectangular box at the edges of each skeleton.
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: Left panel: the H I mass function. The magenta dashed line is ALFALFA’s result. The orange solid line is derived from GAMA LF. The black-shaded region and solid line are derived from our LF with and without cataclysmic variable (CV) correction respectively. The gray-shaded region shows the mass range suffering from sample incompleteness. Right panel: the orange solid line is the GAMA LF. The brown and cyan points with errorbars represent the LF of Blanton et al. (2005), derived by SWML and ﹩1/{V}_{\max }﹩ method respectively. The dark region and points show our LF with and without CV correction.
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: The H I mass in dark matter halos under different luminosity limits. In each panel, the black points represent the average H I mass of all galaxies in halos derived using group catalog. The horizontal black dotted line shows the result of Guo et al. (2020). The red–blue–green–orange lines represent the H I mass in red–blue, central–satellite galaxies from our CHIMFs. The pink upward arrows show the result in the Virgo cluster.
Paper: The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2
Authors: Jihye Hwang, Jongsoo Kim, Kate Pattle, Chang Won Lee, Patrick M. Koch, Doug Johnstone, Kohji Tomisaka, Anthony Whitworth, Ray S. Furuya, Ji-hyun Kang, A-Ran Lyo, Eun Jung Chung, Doris Arzoumanian, Geumsook Park, Woojin Kwon, Shinyoung Kim, Motohide Tamura, Jungmi Kwon, Archana Soam, Ilseung Han, Thiem Hoang, Kyoung Hee Kim, Takashi Onaka, Chakali Eswaraiah, Derek Ward-Thompson, Hong-Li Liu, Xindi Tang, Wen Ping Chen, Masafumi Matsumura, Thuong Duc Hoang, Zhiwei Chen, Valentin J. M. Le Gouellec, Florian Kirchschlager, Frédérick Poidevin, Pierre Bastien, Keping Qiu, Tetsuo Hasegawa, Shih-Ping Lai, Do-Young Byun, Jungyeon Cho, Minho Choi, Youngwoo Choi, Yunhee Choi, Il-Gyo Jeong, Miju Kang, Hyosung Kim, Kee-Tae Kim, Jeong-Eun Lee, Sang-Sung Lee, Yong-Hee Lee, Hyeseung Lee, Mi-Ryang Kim, Hyunju Yoo, Hyeong-Sik Yun, Mike Chen, James Di Francesco, Jason Fiege, Laura M. Fissel, Erica Franzmann, Martin Houde, Kevin Lacaille, Brenda Matthews, Sarah Sadavoy, Gerald Moriarty-Schieven, Mehrnoosh Tahani, Tao-Chung Ching, Y. Sophia Dai, Yan Duan, Qilao Gu, Chi-Yan Law, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Tie Liu, Xing Lu, Lei Qian, Hongchi Wang, Jintai Wu, Jinjin Xie, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Yapeng Zhang, Jianjun Zhou, Lei Zhu, David Berry, Per Friberg, Sarah Graves, Junhao Liu, Steve Mairs, Harriet Parsons, Mark Rawlings, Yasuo Doi, Saeko Hayashi, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Akimasa Kataoka, Koji Kawabata, Gwanjeong Kim, Masato I. N. Kobayashi, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Tae-Soo Pyo, Hiro Saito, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Yusuke Tsukamoto, Tetsuya Zenko, Huei-Ru Vivien Chen, Hao-Yuan Duan, Lapo Fanciullo, Francisca Kemper, Chin-Fei Lee, Sheng-Jun Lin, Sheng-Yuan Liu, Nagayoshi Ohashi, Ramprasad Rao, Ya-Wen Tang, Jia-Wei Wang, Meng-Zhe Yang, Hsi-Wei Yen, Tyler L. Bourke, Antonio Chrysostomou, Victor Debattista, David Eden, Stewart Eyres, Sam Falle, Gary Fuller, Tim Gledhill, Jane Greaves, Matt Griffin, Jennifer Hatchell, Janik Karoly, Jason Kirk, Vera Könyves, Steven Longmore, Sven van Loo, Ilse de Looze, Nicolas Peretto, Felix Priestley, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Giorgio Savini, Anna Scaife, Serena Viti, Pham Ngoc Diep, Nguyen Bich Ngoc, Le Ngoc Tram, Philippe André, Simon Coudé, C. Darren Dowell, Rachel Friesen, Jean-Franćois Robitaille
Figure caption: JCMT HARP C18O (J = 3-2) integrated intensity map in Mon R2. The emission is integrated over the local standard of rest velocity from 6 to 14 km s−1. The contours show SCUBA-2 850 μm flux densities of 0.06, 0.3, 0.6, 1.0, 1.5, 2, 2.5, and 3 Jy beam−1.
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption:                         HST F475W images of the 18 high-confidence sources in our sample, overlaid with FIRST 1.4 GHz contours in the left panel and zoomed-in to highlight the optical morphology of the galaxy in the right panel. All images are centered on the galaxy with north up and east to the left. The restoring beam of the radio map is depicted as a hatched ellipse on the lower-right corner. The radio contours are (−3, 3, 6, 12, 24, 48, 96, ...) × rms of each image, where the values of the rms are listed in Table 3. Object J0847+124 shows an additional 1.5 rms contour in light-gray color. The scale bar in the lower-left corner of each panel indicates the proper distance at the redshift of each object. Figure A1 displays the low-confidence objects.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: In each panel, we show the H I radial profile inferred from the Gault et al. (2021) reported structural parameters as a dashed curve and our estimated radial profile as a solid curve. We also show the directly measured profiles of Leroy et al. (2008) as gray curves in each panel. We find that our estimation method adequately recovers the UDG inferred radial H I profiles, with significantly better performance for inferred profiles close to the average profile—an unsurprising result given that we estimate profiles by assigning galaxies’ average Sérsic parameters for their H I mass.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A comparison between the total stellar mass (left) and SFR (right) estimates derived from our spatially resolved SED fitting if we assume a metallicity of Z = 0.012 (as opposed to our fiducial value of Z = 0.004). In both panels, the gray-filled histogram shows the distribution over all galaxies—the unfilled red and purple histograms show the distribution over the UDG and NSA samples, respectively.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A corner plot of the parameter inference for NSA 7167. As expected, although the 1D distribution of the parameters are strongly peaked and unimodal, there is some degeneracy in the tails of the distribution between the age and amplitude of each component. This can be understood naturally by considering that as the age of a component increases, the mass-to-light ratio drops, meaning that the amplitude of that component (i.e., the stellar mass) must increase to account for the same luminosity.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A comparison of the global SED fits (left column) and joint SED fits (right column) for three galaxies in our sample. In each panel, the red points show the observed fluxes in FUV, NUV, gHSC, rHSC, iHSC, zHSC, and yHSC. Each black curve and set of orange points show the spectrum and synthetic photometry, respectively, of one drawn from the posterior. The text shows the median stellar mass and SFR estimates for each fit; uncertainties correspond to the 16th and 84th percentiles of the posterior.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A sample of three example galaxies from the UDG sample, as labeled. From the left, we show the HSC-SSP gri-composite RGB image, the median SFR surface density map, and the median stellar mass surface density map. These galaxies are chosen to span the range of morphologies present in the sample.
Paper: Grain Growth in the Dust Ring with a Crescent around the Very Low-mass Star ZZ Tau IRS with JVLA
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto
Figure caption: JVLA images (color) overplotted with the ALMA 338.8 GHz image (contour; ﹩{\theta }_{\mathrm{maj}}\times {\theta }_{\min }﹩ = 0.″25×0.″24; P.A. = −62°; Hashimoto et al. 2021a). Contour levels are 0.81 mJy beam−1 (3 σ) × [1, 5, 15]. From left to right the columns show the X-band (8–12 GHz), Ku-band (12–18 GHz), and Ka-band (29–37 GHz) images, respectively. The top row shows the robust = 0 weighted X-band image and the robust = 2 weighted Ku- and K a-band images of ZZ Tau IRS. The middle row shows the images of ZZ Tau that were produced together with those in the top row. The bottom row shows the smoothed, 0.″53 resolution images (refer to Section 2). The synthesized beams of the JVLA observations are shown by the blue ellipses in the lower left corner; the synthesized beam of the ALMA 338.8 image is shown by the white ellipses.
Paper: Grain Growth in the Dust Ring with a Crescent around the Very Low-mass Star ZZ Tau IRS with JVLA
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto
Figure caption: Radial profiles of ZZ Tau IRS and ZZ Tau in top and middle rows in Figure 1, respectively. Vertical dashed line represents the ring location detected in ALMA band 7 dust continuum image (Hashimoto et al. 2021a). The emission of ZZ Tau IRS at 15 and 33 GHz is more spatially extended than those of ZZ Tau, whereas both ZZ Tau IRS and ZZ Tau are not spatially resolved at 10 GHz.
Paper: Grain Growth in the Dust Ring with a Crescent around the Very Low-mass Star ZZ Tau IRS with JVLA
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto
Figure caption: Observed flux densities (dots) from ZZ Tau IRS and our models to interpret them. Panel (a) shows the flux densities measured at the stellar position (i.e., the star column in Table 3). Panel (b) shows the integrated flux densities (i.e., the integrated column in Table 3). In panel (b), the brown and orange lines represent the two dust emission components in our model (i.e., ring and crescent; refer to Table 4), respectively; the dark blue line represents the free–free emission component. The black line represents the total flux density. In panel (a), we only compare the measurements with the free–free emission given that the measurements were drawn from a region that is inside the dust cavity. We note that the off-axis ALMA measurement (green dot) was made well outside of the ALMA primary beam; therefore, it is not reliable.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: Left: H I gas fraction (M H I /M *) vs. stellar mass for our cPSB galaxies in purple, rPSB galaxies in orange, and the ALMaQUEST star-forming galaxies in blue. Downward-pointing triangles represent M H I  upper limits. The dotted and dashed lines show the double power-law fits for LTGs and ETGs from Calette et al. (2018), respectively. Right: molecular-to-atomic gas ratio (﹩{M}_{{{\rm{H}}}_{2}}﹩/M H I ) vs. stellar mass for the same samples. Upward arrows show M H I  upper limits, and downward-pointing arrows show the ﹩{M}_{{{\rm{H}}}_{2}}﹩ upper limits.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: PSD of post-fit residuals for data sets where we individually simulated all binaries (red) and where we simulated a stochastic background and 1000 SMBHBs in each frequency bin (green). We show the median and 90% credible intervals over 200 realizations as solid lines and shaded regions, respectively. The more efficient outlier method correctly reproduces both the median and the variance of the PSD from the full simulations.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: A montage of fitted SFHs through our spectral fitting methods (Section 3.2). In each panel, the MaNGA Plate-IFU, along with several key fitted properties (of only the PSB regions) are listed toward the top right. Their symbols correspond to those in Tables 5 and 3. 8939-3703, highlighted with red text, is found to be a star-forming interloper (see Appendix B). The bottom x-axis traces the age of the universe, with the corresponding redshift scale displayed on the top edge, while the y-axis shows SFRs. The SFHs grow progressively more uncertain with greater lookback time.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: Millimeter and radio emission contours overlaid on SDSS 3-color images for galaxies with 5σ millimeter or radio continuum detections. Green contours show the 3 mm continuum emission, purple contours show the FIRST 1.4 GHz emission, and blue contours show the VLASS 2.4 GHz emission. The ellipses in the lower left of each panel show the beam sizes with the same colors as the contours. Cutout images from the VLASS survey were accessed with astroquery (Ginsburg et al. 2019).
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Distribution of binary parameters in the simulated SMBHB catalog we use. The distribution was artificially cut off below observer-frame GW frequencies of (15 yr)−1, which would not be observable with the 15 yr observing time span considered here. Vertical dashed lines indicate the median value of each parameter.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: CO half-light radii and stellar r-band half-light radii for our PSB sample (centrals in purple, rings in pink) and star-forming galaxies (blue). Galaxies with greater than 50% of CO emission from the central 3σ of the beam are upper limits.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: CO P–V diagrams for each galaxy with a CO detection. The right panel shows the CO velocity field with a dashed line showing the axis where the P–V diagram on the left is extracted from. The color bar is in units of kilometers per second.
Paper: Numerical Simulations of Oscillations in Solar Corona Excited by Vortex Shedding
Authors: Petr Jelínek, Sofya Belov, Marian Karlický
Figure caption: The time evolution of the y-component of vorticity ω, in arbitrary units, showing the oscillations of the structure (black area) for times t ≈ 314, 388, 399, and 526 s, respectively.
Paper: Numerical Simulations of Oscillations in Solar Corona Excited by Vortex Shedding
Authors: Petr Jelínek, Sofya Belov, Marian Karlický
Figure caption: The oscillation signal obtained from the motion of gravity center of the magnetic structure (upper panel) and its wavelet analysis (bottom panel).
Paper: Numerical Simulations of Oscillations in Solar Corona Excited by Vortex Shedding
Authors: Petr Jelínek, Sofya Belov, Marian Karlický
Figure caption: The period of the oscillation of the magnetic structure, obtained from the wavelet analysis.
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: Ultraviolet and blue-optical spectra of G238-44 and models as described in Section 3.1. Low-resolution and high-S/N STIS spectra are displayed for wavelengths longer than 1300 Å in preference to lower-S/N COS spectra; STIS spectra are used as obtained from MAST without further processing. The model produced with nominal values of T eff and log  g is an excellent match to the flux-calibrated spectra.